Hibiki Yama, Kento Masuda, Yui Kawashima, Hajime Kawahara: ExoJAX Retrievals of VLT/CRIRES Spectra of Luhman 16AB: C/O Ratios and Systematic Uncertainties https://arxiv.org/abs/2511.23018 https://arxiv.org/pdf/2511.23018 https://arxiv.org/html/2511.23018
New paper out: Differentiable Microlensing Modeling (led by Shota Miyazaki) arxiv.org/abs/2510.02639
Last week, I gave an intensive course (exoplanets and inference) at Tohoku University. I am sharing the lecture materials here. github.com/HajimeKawaha...
ExoJAX 2.2.0 has been released! We continue to modularize the entire codebase. The differentiable thermochemical equilibrium code ExoGibbs is now under development, and ExoJAX can already be coupled with it. github.com/HajimeKawaha...
Atmospheric asymmetry changes both the central time and duration of the transit light curve
Our paper, led by Shotaro Tada, is out. Atmospheric asymmetry not only affects the central time of the transit but also induces chromatic variations in duration, can be used to know differences in the atmosphere between the dayside and nightside near the limb. arxiv.org/abs/2503.08988
Figure 5: Best fit models to one of one of Enceladus’ phase curves (filter 798 nm) for three different models: a pure single Henyey-Greenstein model with no additional opposition peak, shadow hiding model, and coherent backscattering model. Top panel shows the fits and the second panel shows the residuals of these best fits. It is clear that the model with no opposition peak is the worst fit to the data. The other two models produce, by eye, almost identical fits, which is expected since the functional forms are similar. However the residuals still show subtle differences. Using the LOO model selection statistic allows us to conclude that the coherent backscattering model is preferred by 7/12 of the phase curves, however not significantly. The corner plot showing the posteriors for the shadow hiding model are in Appendix A, Figure A.2.
*Newly Dr.* Kathryn Jones (+me and Kevin Heng) asks: "Planets show a sharp surge in brightness when directly opposite the Sun, and this peak is sharper for solid planets than for gas planets. Could we use this to detect rocky surfaces with JWST or HWO?" 🧪🔭🪐
tl;dr: no.
arxiv.org/abs/2502.14629
